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Start Over Author "Cortese, L." Journal monthly notices of the royal astronomical society
202 results on '"Cortese, L."'

1. WALLABY pilot survey: an ‘almost’ dark cloud near the Hydra cluster

Author

O’Beirne, T, primary, Staveley-Smith, L, additional, Wong, O I, additional, Westmeier, T, additional, Batten, G, additional, Kilborn, V A, additional, Lee-Waddell, K, additional, Mancera Piña, P E, additional, Román, J, additional, Verdes-Montenegro, L, additional, Catinella, B, additional, Cortese, L, additional, Deg, N, additional, Dénes, H, additional, For, B Q, additional, Kamphuis, P, additional, Koribalski, B S, additional, Murugeshan, C, additional, Rhee, J, additional, Spekkens, K, additional, Wang, J, additional, Bekki, K, additional, and Lṕpez-Sánchez, Á R, additional

Published
2024
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3. PACS photometry of the Herschel Reference Survey – far-infrared/submillimetre colours as tracers of dust properties in nearby galaxies

Author

Cortese, L, Fritz, J, Bianchi, S, Boselli, A, Ciesla, L, Bendo, GJ, Boquien, M, Roussel, H, Baes, M, Buat, V, Clemens, M, Cooray, A, Cormier, D, Davies, JI, De Looze, I, Eales, SA, Fuller, C, Hunt, LK, Madden, S, Munoz-Mateos, J, Pappalardo, C, Pierini, D, Rémy-Ruyer, A, Sauvage, M, di Serego Alighieri, S, Smith, MWL, Spinoglio, L, Vaccari, M, and Vlahakis, C

Subjects
galaxies: fundamental parameters, galaxies: ISM, infrared: galaxies, astro-ph.GA, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We present Herschel/PACS 100 and 160 μm integrated photometry for the 323 galaxies in the Herschel Reference Survey (HRS), a K-band, volume-limited sample of galaxies in the local Universe. Once combined with the Herschel/SPIRE observations already available, these data make the HRS the largest representative sample of nearby galaxies with homogeneous coverage across the 100-500 μm wavelength range. In this paper, we take advantage of this unique data set to investigate the properties and shape of the far-infrared/submillimetre spectral energy distribution in nearby galaxies. We show that, in the stellar mass range covered by the HRS (8 ≤ log (M*/M⊙) ≤ 12), the far-infrared/submillimetre colours are inconsistent with a single modified blackbody having the same dust emissivity index β for all galaxies. In particular, either β decreases or multiple temperature components are needed, when moving from metal-rich/gas-poor to metal-poor/gas-rich galaxies. We thus investigate how the dust temperature and mass obtained from a single modified blackbody depend on the assumptions made on β. We show that, while the correlations between dust temperature, galaxy structure and star formation rate are strongly model dependent, the dust mass scaling relations are much more reliable, and variations of β only change the strength of the observed trends. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Published
2014

4. WALLABY pilot survey: an 'almost' dark cloud near the Hydra cluster.

Author

O'Beirne, T, Staveley-Smith, L, Wong, O I, Westmeier, T, Batten, G, Kilborn, V A, Lee-Waddell, K, Mancera Piña, P E, Román, J, Verdes-Montenegro, L, Catinella, B, Cortese, L, Deg, N, Dénes, H, For, B Q, Kamphuis, P, Koribalski, B S, Murugeshan, C, Rhee, J, and Spekkens, K

Subjects
WALLABIES, DARK energy, OPTICAL limiting, DATA release, GALACTIC evolution
Abstract

We explore the properties of an 'almost' dark cloud of neutral hydrogen (H  i) using data from the Widefield ASKAP L-band Legacy All-sky Survey (WALLABY). Until recently, WALLABY J103508 − 283427 (also known as H1032 − 2819 or LEDA 2793457) was not known to have an optical counterpart, but we have identified an extremely faint optical counterpart in the Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Survey Data Release 10. We measured the mean g -band surface brightness to be 27.0 ± 0.3 mag arcsec−2. The WALLABY data revealed the cloud to be closely associated with the interacting group Klemola 13 (also known as HIPASS J1034 − 28 and the Tol 9 group), which itself is associated with the Hydra cluster. In addition to WALLABY J103508 − 283427/H1032 − 2819, Klemola 13 contains 10 known significant galaxies and almost half of the total H  i gas is beyond the optical limits of the galaxies. By combining the new WALLABY data with archival data from the Australia Telescope Compact Array, we investigate the H  i distribution and kinematics of the system. We discuss the relative role of tidal interactions and ram pressure stripping in the formation of the cloud and the evolution of the system. The ease of detection of this cloud and intragroup gas is due to the sensitivity, resolution, and wide field of view of WALLABY, and showcases the potential of the full WALLABY survey to detect many more examples. [ABSTRACT FROM AUTHOR]

Published
2024
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5. The Tully–Fisher relation from SDSS-MaNGA: physical causes of scatter and variation at different radii.

Author

Ristea, A, Cortese, L, Fraser-McKelvie, A, Catinella, B, van de Sande, J, Croom, S M, and Swinbank, A M

Subjects
*STELLAR rotation, *GALACTIC evolution, *IONIZED gases, *STARS, *STAR formation
Abstract

The stellar mass Tully–Fisher relation (STFR) and its scatter encode valuable information about the processes shaping galaxy evolution across cosmic time. However, we are still missing a proper quantification of the STFR slope and scatter dependence on the baryonic tracer used to quantify rotational velocity, on the velocity measurement radius and on galaxy integrated properties. We present a catalogue of stellar and ionized gas (traced by H |$\rm {\alpha }$| emission) kinematic measurements for a sample of galaxies drawn from the MaNGA Galaxy Survey, providing an ideal tool for galaxy formation model calibration and for comparison with high-redshift studies. We compute the STFRs for stellar and gas rotation at 1, 1.3 and 2 effective radii (R e). The relations for both baryonic components become shallower at 2 R e compared to 1 R e and 1.3 R e. We report a steeper STFR for the stars in the inner parts (≤1.3 R e) compared to the gas. At 2 R e, the relations for the two components are consistent. When accounting for covariances with integrated v /σ, scatter in the stellar and gas STFRs shows no strong correlation with: optical morphology, star formation rate surface density, tidal interaction strength or gas accretion signatures. Our results suggest that the STFR scatter is driven by an increase in stellar/gas dispersional support, from either external (mergers) or internal (feedback) processes. No correlation between STFR scatter and environment is found. Nearby Universe galaxies have their stars and gas in statistically different states of dynamical equilibrium in the inner parts (≤1.3 R e), while at 2 R e the two components are dynamically coupled. [ABSTRACT FROM AUTHOR]

Published
2024
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9. WALLABY pilot survey: H i gas disc truncation and star formation of galaxies falling into the Hydra I cluster

Author

Reynolds, T N, primary, Catinella, B, additional, Cortese, L, additional, Westmeier, T, additional, Meurer, G R, additional, Shao, L, additional, Obreschkow, D, additional, Román, J, additional, Verdes-Montenegro, L, additional, Deg, N, additional, Dénes, H, additional, For, B-Q, additional, Kleiner, D, additional, Koribalski, B S, additional, Lee-Waddell, K, additional, Murugeshan, C, additional, Oh, S-H, additional, Rhee, J, additional, Spekkens, K, additional, Staveley-Smith, L, additional, Stevens, A R H, additional, van der Hulst, J M, additional, Wang, J, additional, Wong, O I, additional, Holwerda, B W, additional, Bosma, A, additional, Madrid, J P, additional, and Bekki, K, additional

Published
2021
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10. The SAMI Galaxy Survey: the drivers of gas and stellar metallicity differences in galaxies

Author

Fraser-McKelvie, A, primary, Cortese, L, additional, Groves, B, additional, Brough, S, additional, Bryant, J, additional, Catinella, B, additional, Croom, S, additional, D’Eugenio, F, additional, López-Sánchez, Á R, additional, van de Sande, J, additional, Sweet, S, additional, Vaughan, S, additional, Bland-Hawthorn, J, additional, Lawrence, J, additional, Lorente, N, additional, and Owers, M, additional

Published
2021
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11. Deep Extragalactic VIsible Legacy Survey (DEVILS): evolution of the σSFR–M⋆ relation and implications for self-regulated star formation

Author

Davies, L J M, primary, Thorne, J E, additional, Bellstedt, S, additional, Bravo, M, additional, Robotham, A S G, additional, Driver, S P, additional, Cook, R H W, additional, Cortese, L, additional, D’Silva, J, additional, Grootes, M W, additional, Holwerda, B W, additional, Hopkins, A M, additional, Jarvis, M J, additional, Lidman, C, additional, Phillipps, S, additional, and Siudek, M, additional

Published
2021
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12. SAMI Galaxy Survey: physical drivers of stellar-gas kinematic misalignments in the nearby Universe.

Author

Ristea, A, Cortese, L, Fraser-McKelvie, A, Brough, S, Bryant, J J, Catinella, B, Croom, S M, Groves, B, Richards, S N, van de Sande, J, Bland-Hawthorn, J, Owers, M S, and Lawrence, J S

Subjects
*GALACTIC evolution, *STELLAR rotation, *DRAG force, *STAR formation, UNIVERSE
Abstract

Misalignments between the rotation axis of stars and gas are an indication of external processes shaping galaxies throughout their evolution. Using observations of 3068 galaxies from the SAMI Galaxy Survey, we compute global kinematic position angles for 1445 objects with reliable kinematics and identify 169 (12 per cent) galaxies which show stellar-gas misalignments. Kinematically decoupled features are more prevalent in early-type/passive galaxies compared to late-type/star-forming systems. Star formation is the main source of gas ionization in only 22 per cent of misaligned galaxies; 17 per cent are Seyfert objects, while 61 per cent show Low-Ionization Nuclear Emission-line Region features. We identify the most probable physical cause of the kinematic decoupling and find that, while accretion-driven cases are dominant, for up to 8 per cent of our sample, the misalignment may be tracing outflowing gas. When considering only misalignments driven by accretion, the acquired gas is feeding active star formation in only ∼1/4 of cases. As a population, misaligned galaxies have higher Sérsic indices and lower stellar spin and specific star formation rates than appropriately matched samples of aligned systems. These results suggest that both morphology and star formation/gas content are significantly correlated with the prevalence and timescales of misalignments. Specifically, torques on misaligned gas discs are smaller for more centrally concentrated galaxies, while the newly accreted gas feels lower viscous drag forces in more gas-poor objects. Marginal evidence of star formation not being correlated with misalignment likelihood for late-type galaxies suggests that such morphologies in the nearby Universe might be the result of preferentially aligned accretion at higher redshifts. [ABSTRACT FROM AUTHOR]

Published
2022
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14. Deep Extragalactic VIsible Legacy Survey (DEVILS): consistent multiwavelength photometry for the DEVILS regions (COSMOS, XMMLSS, and ECDFS)

Author

Davies, L J M, primary, Thorne, J E, additional, Robotham, A S G, additional, Bellstedt, S, additional, Driver, S P, additional, Adams, N J, additional, Bilicki, M, additional, Bowler, R A A, additional, Bravo, M, additional, Cortese, L, additional, Foster, C, additional, Grootes, M W, additional, Häußler, B, additional, Hashemizadeh, A, additional, Holwerda, B W, additional, Hurley, P, additional, Jarvis, M J, additional, Lidman, C, additional, Maddox, N, additional, Meyer, M, additional, Paolillo, M, additional, Phillipps, S, additional, Radovich, M, additional, Siudek, M, additional, Vaccari, M, additional, and Windhorst, R A, additional

Published
2021
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15. The SAMI Galaxy Survey: the role of disc fading and progenitor bias in kinematic transitions

Author

Croom, S M, primary, Taranu, D S, additional, van de Sande, J, additional, Lagos, C D P, additional, Harborne, K E, additional, Bland-Hawthorn, J, additional, Brough, S, additional, Bryant, J J, additional, Cortese, L, additional, Foster, C, additional, Goodwin, M, additional, Groves, B, additional, Khalid, A, additional, Lawrence, J, additional, Medling, A M, additional, Richards, S N, additional, Owers, M S, additional, Scott, N, additional, and Vaughan, S P, additional

Published
2021
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16. WALLABY pilot survey: first look at the Hydra I cluster and ram pressure stripping of ESO 501−G075

Author

Reynolds, T N, primary, Westmeier, T, additional, Elagali, A, additional, Catinella, B, additional, Cortese, L, additional, Deg, N, additional, For, B-Q, additional, Kamphuis, P, additional, Kleiner, D, additional, Koribalski, B S, additional, Lee-Waddell, K, additional, Oh, S-H, additional, Rhee, J, additional, Serra, P, additional, Spekkens, K, additional, Staveley-Smith, L, additional, Stevens, A R H, additional, Taylor, E N, additional, Wang, J, additional, and Wong, O I, additional

Published
2021
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17. physical connection between central stellar surface density and stellar spin in SAMI and MaNGA nearby galaxies.

Author

Cortese, L, Fraser-McKelvie, A, Woo, J, Catinella, B, Harborne, K E, van de Sande, J, Bland-Hawthorn, J, Brough, S, Bryant, J J, Croom, S, and Sweet, S

Subjects
*GALAXIES, *STAR formation, *ASTRONOMICAL surveys, *GALACTIC evolution, *DENSITY, *STELLAR mass, *GALACTIC bulges
Abstract

The stellar surface density within the inner 1 kpc (Σ1) has become a popular tool for understanding the growth of galaxies and its connection with the quenching of star formation. The emerging picture suggests that building a central dense core is a necessary condition for quenching. However, it is not clear whether changes in Σ1 trace changes in stellar kinematics and the growth of dispersion-dominated bulges. In this paper, we combine imaging from the Sloan Digital Sky Survey with stellar kinematics from the Sydney-AAO Multi-object Integral-field unit and Mapping Nearby Galaxies at Apache Point Observatory surveys to quantify the correlation between Σ1 and the proxy for stellar spin parameter within one effective radius (λre) for 1599 nearby galaxies. We show that, on the star-forming main sequence and at fixed stellar mass, changes in Σ1 are mirrored by changes in λre. While forming stars, main-sequence galaxies remain rotationally-dominated systems, with their Σ1 increasing but their stellar spin staying either constant or slightly increasing. The picture changes below the main sequence, where Σ1 and λre are no longer correlated. Passive systems show a narrower range of Σ1, but a wider range of λre compared to star-forming galaxies. Our results indicate that, from a structural point of view, passive galaxies are a more heterogeneous population than star-forming systems, and may have followed a variety of evolutionary paths. This also suggests that, if dispersion-dominated bulges still grow significantly at z ∼ 0, this generally takes place during, or after, the quenching phase. [ABSTRACT FROM AUTHOR]

Published
2022
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18. A SAMI and MaNGA view on the stellar kinematics of galaxies on the star-forming main sequence

Author

Fraser-McKelvie, A, primary, Cortese, L, additional, van de Sande, J, additional, Bryant, J J, additional, Catinella, B, additional, Colless, M, additional, Croom, S M, additional, Groves, B, additional, Medling, A M, additional, Scott, N, additional, Sweet, S M, additional, Bland-Hawthorn, J, additional, Goodwin, M, additional, Lawrence, J, additional, Lorente, N, additional, Owers, M S, additional, and Richards, S N, additional

Published
2021
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19. Centrally concentrated molecular gas driving galactic-scale ionized gas outflows in star-forming galaxies

Author

Hogarth, L M, primary, Saintonge, A, additional, Cortese, L, additional, Davis, T A, additional, Croom, S M, additional, Bland-Hawthorn, J, additional, Brough, S, additional, Bryant, J J, additional, Catinella, B, additional, Fletcher, T J, additional, Groves, B, additional, Lawrence, J S, additional, López-Sánchez, Á R, additional, Owers, M S, additional, Richards, S N, additional, Roberts-Borsani, G W, additional, Taylor, E N, additional, van de Sande, J, additional, and Scott, N, additional

Published
2020
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20. WALLABY pilot survey: H i gas disc truncation and star formation of galaxies falling into the Hydra I cluster.

Author

Reynolds, T N, Catinella, B, Cortese, L, Westmeier, T, Meurer, G R, Shao, L, Obreschkow, D, Román, J, Verdes-Montenegro, L, Deg, N, Dénes, H, For, B-Q, Kleiner, D, Koribalski, B S, Lee-Waddell, K, Murugeshan, C, Oh, S-H, Rhee, J, Spekkens, K, and Staveley-Smith, L

Subjects
GALAXY formation, STAR formation, WALLABIES, GALAXY clusters, GAS reservoirs, ATOMIC hydrogen
Abstract

We present results from our analysis of the Hydra I cluster observed in neutral atomic hydrogen (H  i) as part of the Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY). These WALLABY observations cover a 60-square-degree field of view with uniform sensitivity and a spatial resolution of 30 arcsec. We use these wide-field observations to investigate the effect of galaxy environment on H  i gas removal and star formation quenching by comparing the properties of cluster, infall, and field galaxies extending up to ∼5 R 200 from the cluster centre. We find a sharp decrease in the H  i -detected fraction of infalling galaxies at a projected distance of ∼1.5 R 200 from the cluster centre from |$\sim 85{{\ \rm per\ cent}}$| to |$\sim 35{{\ \rm per\ cent}}$|⁠. We see evidence for the environment removing gas from the outskirts of H  i -detected cluster and infall galaxies through the decrease in the H  i to r -band optical disc diameter ratio. These galaxies lie on the star-forming main sequence, indicating that gas removal is not yet affecting the inner star-forming discs and is limited to the galaxy outskirts. Although we do not detect galaxies undergoing galaxy-wide quenching, we do observe a reduction in recent star formation in the outer disc of cluster galaxies, which is likely due to the smaller gas reservoirs present beyond the optical radius in these galaxies. Stacking of H  i non-detections with H  i masses below |$M_{\rm {HI}}\lesssim 10^{8.4}\, \rm {M}_{\odot }$| will be required to probe the H  i of galaxies undergoing quenching at distances ≳60 Mpc with WALLABY. [ABSTRACT FROM AUTHOR]

Published
2022
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21. SAMI Galaxy Survey: the drivers of gas and stellar metallicity differences in galaxies.

Author

Fraser-McKelvie, A, Cortese, L, Groves, B, Brough, S, Bryant, J, Catinella, B, Croom, S, D'Eugenio, F, López-Sánchez, Á R, van de Sande, J, Sweet, S, Vaughan, S, Bland-Hawthorn, J, Lawrence, J, Lorente, N, and Owers, M

Subjects
*GALAXIES, *GALACTIC evolution, *INTERSTELLAR medium, *GRAVITATIONAL potential, *GALAXY formation
Abstract

The combination of gas-phase oxygen abundances and stellar metallicities can provide us with unique insights into the metal enrichment histories of galaxies. In this work, we compare the stellar and gas-phase metallicities measured within a 1 Re aperture for a representative sample of 472 star-forming galaxies extracted from the SAMI Galaxy Survey. We confirm that the stellar and interstellar medium (ISM) metallicities are strongly correlated, with scatter ∼3 times smaller than that found in previous works, and that integrated stellar populations are generally more metal-poor than the ISM, especially in low-mass galaxies. The ratio between the two metallicities strongly correlates with several integrated galaxy properties including stellar mass, specific star formation rate, and a gravitational potential proxy. However, we show that these trends are primarily a consequence of: (a) the different star formation and metal enrichment histories of the galaxies, and (b) the fact that while stellar metallicities trace primarily iron enrichment, gas-phase metallicity indicators are calibrated to the enrichment of oxygen in the ISM. Indeed, once both metallicities are converted to the same 'element base' all of our trends become significantly weaker. Interestingly, the ratio of gas to stellar metallicity is always below the value expected for a simple closed-box model, which requires that outflows and inflows play an important role in the enrichment history across our entire stellar mass range. This work highlights the complex interplay between stellar and gas-phase metallicities and shows how care must be taken in comparing them to constrain models of galaxy formation and evolution. [ABSTRACT FROM AUTHOR]

Published
2022
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23. From peculiar morphologies to Hubble-type spirals: the relation between galaxy dynamics and morphology in star-forming galaxies at z ∼ 1.5

Author

Gillman, S, primary, Tiley, A L, additional, Swinbank, A M, additional, Harrison, C M, additional, Smail, Ian, additional, Dudzevičiūtė, U, additional, Sharples, R M, additional, Cortese, L, additional, Obreschkow, D, additional, Bower, R G, additional, Theuns, T, additional, Cirasuolo, M, additional, Fisher, D B, additional, Glazebrook, K, additional, Ibar, Edo, additional, Mendel, J Trevor, additional, and Sweet, Sarah M, additional

Published
2019
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24. The SAMI Galaxy Survey: first detection of a transition in spin orientation with respect to cosmic filaments in the stellar kinematics of galaxies

Author

Welker, C, primary, Bland-Hawthorn, J, additional, Van de Sande, J, additional, Lagos, C, additional, Elahi, P, additional, Obreschkow, D, additional, Bryant, J, additional, Pichon, C, additional, Cortese, L, additional, Richards, S N, additional, Croom, S M, additional, Goodwin, M, additional, Lawrence, J S, additional, Sweet, S, additional, Lopez-Sanchez, A, additional, Medling, A, additional, Owers, M S, additional, Dubois, Y, additional, and Devriendt, J, additional

Published
2019
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25. WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

Author

For, B-Q, primary, Staveley-Smith, L, additional, Westmeier, T, additional, Whiting, M, additional, Oh, S-H, additional, Koribalski, B, additional, Wang, J, additional, Wong, O I, additional, Bekiaris, G, additional, Cortese, L, additional, Elagali, A, additional, Kleiner, D, additional, Lee-Waddell, K, additional, Madrid, J P, additional, Popping, A, additional, Rhee, J, additional, Reynolds, T N, additional, Collier, J D, additional, Phillips, C J, additional, Voronkov, M A, additional, Müller, O, additional, and Jerjen, H, additional

Published
2019
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27. Galaxy And Mass Assembly (GAMA): Environmental Quenching of Centrals and Satellites in Groups

Author

Davies, L J M, primary, Robotham, A S G, additional, Lagos, C del P, additional, Driver, S P, additional, Stevens, A R H, additional, Bahé, Y M, additional, Alpaslan, M, additional, Bremer, M N, additional, Brown, M J I, additional, Brough, S, additional, Bland-Hawthorn, J, additional, Cortese, L, additional, Elahi, P, additional, Grootes, M W, additional, Holwerda, B W, additional, Ludlow, A D, additional, McGee, S, additional, Owers, M, additional, and Phillipps, S, additional

Published
2019
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28. The SAMI Galaxy Survey: observing the environmental quenching of star formation in GAMA groups

Author

Schaefer, A L, primary, Croom, S M, additional, Scott, N, additional, Brough, S, additional, Allen, J T, additional, Bekki, K, additional, Bland-Hawthorn, J, additional, Bloom, J V, additional, Bryant, J J, additional, Cortese, L, additional, Davies, L J M, additional, Federrath, C, additional, Fogarty, L M R, additional, Green, A W, additional, Groves, B, additional, Hopkins, A M, additional, Konstantopoulos, I S, additional, López-Sánchez, A R, additional, Lawrence, J S, additional, McElroy, R E, additional, Medling, A M, additional, Owers, M S, additional, Pracy, M B, additional, Richards, S N, additional, Robotham, A S G, additional, van de Sande, J, additional, Tonini, C, additional, and Yi, S K, additional

Published
2018
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29. The SAMI Galaxy Survey: stellar and gas misalignments and the origin of gas in nearby galaxies

Author

Bryant, J J, primary, Croom, S M, additional, van de Sande, J, additional, Scott, N, additional, Fogarty, L M R, additional, Bland-Hawthorn, J, additional, Bloom, J V, additional, Taylor, E N, additional, Brough, S, additional, Robotham, A, additional, Cortese, L, additional, Couch, W, additional, Owers, M S, additional, Medling, A M, additional, Federrath, C, additional, Bekki, K, additional, Richards, S N, additional, Lawrence, J S, additional, and Konstantopoulos, I S, additional

Published
2018
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31. Galaxy And Mass Assembly (GAMA): The sSFR-M* relation part I – σsSFR-M* as a function of sample, SFR indicator and environment

Author

Davies, L J M, primary, del P Lagos, C, additional, Katsianis, A, additional, Robotham, A S G, additional, Cortese, L, additional, Driver, S P, additional, Bremer, M N, additional, Brown, M J I, additional, Brough, S, additional, Cluver, M E, additional, Grootes, M W, additional, Holwerda, B W, additional, Owers, M, additional, and Phillipps, S, additional

Published
2018
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32. From peculiar morphologies to Hubble-type spirals: the relation between galaxy dynamics and morphology in star-forming galaxies at z ∼ 1.5.

Author

Gillman, S, Tiley, A L, Swinbank, A M, Harrison, C M, Smail, Ian, Dudzevičiūtė, U, Sharples, R M, Cortese, L, Obreschkow, D, Bower, R G, Theuns, T, Cirasuolo, M, Fisher, D B, Glazebrook, K, Ibar, Edo, Mendel, J Trevor, and Sweet, Sarah M

Subjects
GALACTIC dynamics, STELLAR mass, GAS dynamics, GALAXIES, ANGULAR momentum (Mechanics), STAR formation
Abstract

We present an analysis of the gas dynamics of star-forming galaxies at z ∼ 1.5 using data from the KMOS Galaxy Evolution Survey. We quantify the morphology of the galaxies using HST candels imaging parametrically and non-parametrically. We combine the H α dynamics from KMOS with the high-resolution imaging to derive the relation between stellar mass (M *) and stellar specific angular momentum (j *). We show that high-redshift star-forming galaxies at z ∼ 1.5 follow a power-law trend in specific stellar angular momentum with stellar mass similar to that of local late-type galaxies of the form j *  ∝   M |$_*^{0.53\, \pm \, 0.10}$|⁠. The highest specific angular momentum galaxies are mostly disc-like, although generally both peculiar morphologies and disc-like systems are found across the sequence of specific angular momentum at a fixed stellar mass. We explore the scatter within the j * –  M * plane and its correlation with both the integrated dynamical properties of a galaxy (e.g. velocity dispersion, Toomre Qg, H α star formation rate surface density ΣSFR) and its parametrized rest-frame UV / optical morphology (e.g. Sérsic index, bulge to total ratio, clumpiness, asymmetry, and concentration). We establish that the position in the j * –  M * plane is strongly correlated with the star-formation surface density and the clumpiness of the stellar light distribution. Galaxies with peculiar rest-frame UV / optical morphologies have comparable specific angular momentum to disc- dominated galaxies of the same stellar mass, but are clumpier and have higher star formation rate surface densities. We propose that the peculiar morphologies in high-redshift systems are driven by higher star formation rate surface densities and higher gas fractions leading to a more clumpy interstellar medium. [ABSTRACT FROM AUTHOR]

Published
2020
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33. The SAMI Galaxy Survey: first detection of a transition in spin orientation with respect to cosmic filaments in the stellar kinematics of galaxies.

Author

Welker, C, Bland-Hawthorn, J, Van de Sande, J, Lagos, C, Elahi, P, Obreschkow, D, Bryant, J, Pichon, C, Cortese, L, Richards, S N, Croom, S M, Goodwin, M, Lawrence, J S, Sweet, S, Lopez-Sanchez, A, Medling, A, Owers, M S, Dubois, Y, and Devriendt, J

Subjects
GALAXY formation, SPIN crossover, FIBERS, GALAXIES, STELLAR mergers, KINEMATICS
Abstract

We present the first detection of mass-dependent galactic spin alignments with local cosmic filaments with >2σ confidence using IFS kinematics. The 3D network of cosmic filaments is reconstructed on Mpc scales across GAlaxy and Mass Assembly fields using the cosmic web extractor DisPerSe. We assign field galaxies from the SAMI survey to their nearest filament segment in 3D and estimate the degree of alignment between SAMI galaxies' kinematic spin axis and their nearest filament in projection. Low-mass galaxies align their spin with their nearest filament while higher mass counterparts are more likely to display an orthogonal orientation. The stellar transition mass from the first trend to the second is bracketed between |$10^{10.4}$| and |$10^{10.9}\, \mathrm{ M}_{\odot }$|⁠ , with hints of an increase with filament scale. Consistent signals are found in the Horizon-AGN cosmological hydrodynamic simulation. This supports a scenario of early angular momentum build-up in vorticity rich quadrants around filaments at low stellar mass followed by progressive flip of spins orthogonal to the cosmic filaments through mergers at high stellar mass. Conversely, we show that dark matter only simulations post-processed with a semi-analytical model treatment of galaxy formation struggles to reproduce this alignment signal. This suggests that gas physics is key in enhancing the galaxy-filament alignment. [ABSTRACT FROM AUTHOR]

Published
2020
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34. KROSS–SAMI: a direct IFS comparison of the Tully–Fisher relation across 8 Gyr sincez ≈ 1

Author

Tiley, A L, primary, Bureau, M, additional, Cortese, L, additional, Harrison, C M, additional, Johnson, H L, additional, Stott, J P, additional, Swinbank, A M, additional, Smail, I, additional, Sobral, D, additional, Bunker, A J, additional, Glazebrook, K, additional, Bower, R G, additional, Obreschkow, D, additional, Bryant, J J, additional, Jarvis, M J, additional, Bland-Hawthorn, J, additional, Magdis, G, additional, Medling, A M, additional, Sweet, S M, additional, Tonini, C, additional, Turner, O J, additional, Sharples, R M, additional, Croom, S M, additional, Goodwin, M, additional, Konstantopoulos, I S, additional, Lorente, N P F, additional, Lawrence, J S, additional, Mould, J, additional, Owers, M S, additional, and Richards, S N, additional

Published
2018
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35. The SAMI Galaxy Survey: embedded discs and radial trends in outer dynamical support across the Hubble sequence

Author

Foster, C, primary, van de Sande, J, additional, Cortese, L, additional, Croom, S M, additional, Bland-Hawthorn, J, additional, Brough, S, additional, Bryant, J J, additional, Goodwin, M, additional, Lawrence, J S, additional, Lorente, N, additional, Medling, A M, additional, Owers, M, additional, Richards, S N, additional, and Scott, N, additional

Published
2018
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36. Deep Extragalactic VIsible Legacy Survey (DEVILS): motivation,design, and target catalogue

Author

Davies, L J M, primary, Robotham, A S G, additional, Driver, S P, additional, Lagos, C P, additional, Cortese, L, additional, Mannering, E, additional, Foster, C, additional, Lidman, C, additional, Hashemizadeh, A, additional, Koushan, S, additional, O’Toole, S, additional, Baldry, I K, additional, Bilicki, M, additional, Bland-Hawthorn, J, additional, Bremer, M N, additional, Brown, M J I, additional, Bryant, J J, additional, Catinella, B, additional, Croom, S M, additional, Grootes, M W, additional, Holwerda, B W, additional, Jarvis, M J, additional, Maddox, N, additional, Meyer, M, additional, Moffett, A J, additional, Phillipps, S, additional, Taylor, E N, additional, Windhorst, R A, additional, and Wolf, C, additional

Published
2018
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37. The SAMI Galaxy Survey: gas content and interaction as the drivers of kinematic asymmetry

Author

Bloom, J V, primary, Croom, S M, additional, Bryant, J J, additional, Schaefer, A L, additional, Bland-Hawthorn, J, additional, Brough, S, additional, Callingham, J, additional, Cortese, L, additional, Federrath, C, additional, Scott, N, additional, van de Sande, J, additional, D'Eugenio, F, additional, Sweet, S, additional, Tonini, C, additional, Allen, J T, additional, Goodwin, M, additional, Green, A W, additional, Konstantopoulos, I S, additional, Lawrence, J, additional, Lorente, N, additional, Medling, A M, additional, Owers, M S, additional, Richards, S N, additional, and Sharp, R, additional

Published
2018
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40. The KMOS Redshift One Spectroscopic Survey (KROSS): the origin of disc turbulence in z ≈ 1 star-forming galaxies

Author

Johnson, H L, primary, Harrison, C M, additional, Swinbank, A M, additional, Tiley, A L, additional, Stott, J P, additional, Bower, R G, additional, Smail, Ian, additional, Bunker, A J, additional, Sobral, D, additional, Turner, O J, additional, Best, P, additional, Bureau, M, additional, Cirasuolo, M, additional, Jarvis, M J, additional, Magdis, G, additional, Sharples, R M, additional, Bland-Hawthorn, J, additional, Catinella, B, additional, Cortese, L, additional, Croom, S M, additional, Federrath, C, additional, Glazebrook, K, additional, Sweet, S M, additional, Bryant, J J, additional, Goodwin, M, additional, Konstantopoulos, I S, additional, Lawrence, J S, additional, Medling, A M, additional, Owers, M S, additional, and Richards, S, additional

Published
2017
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41. Tidal origin of NGC 1427A in the Fornax cluster

Author

Lee-Waddell, K., primary, Serra, P., additional, Koribalski, B., additional, Venhola, A., additional, Iodice, E., additional, Catinella, B., additional, Cortese, L., additional, Peletier, R., additional, Popping, A., additional, Keenan, O., additional, and Capaccioli, M., additional

Published
2017
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42. The SAMI Galaxy Survey: understanding observations of large-scale outflows at low redshift with EAGLE simulations

Author

Tescari, E., primary, Cortese, L., additional, Power, C., additional, Wyithe, J. S. B., additional, Ho, I.-T., additional, Crain, R. A., additional, Bland-Hawthorn, J., additional, Croom, S. M., additional, Kewley, L. J., additional, Schaye, J., additional, Bower, R. G., additional, Theuns, T., additional, Schaller, M., additional, Barnes, L., additional, Brough, S., additional, Bryant, J. J., additional, Goodwin, M., additional, Gunawardhana, M. L. P., additional, Lawrence, J. S., additional, Leslie, S. K., additional, López-Sánchez, Á. R., additional, Lorente, N. P. F., additional, Medling, A. M., additional, Richards, S. N., additional, Sweet, S. M., additional, and Tonini, C., additional

Published
2017
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43. The SAMI Galaxy Survey: the intrinsic shape of kinematically selected galaxies

Author

Foster, C., primary, van de Sande, J., additional, D'Eugenio, F., additional, Cortese, L., additional, McDermid, R. M., additional, Bland-Hawthorn, J., additional, Brough, S., additional, Bryant, J., additional, Croom, S. M., additional, Goodwin, M., additional, Konstantopoulos, I. S., additional, Lawrence, J., additional, López-Sánchez, Á. R., additional, Medling, A. M., additional, Owers, M. S., additional, Richards, S. N., additional, Scott, N., additional, Taranu, D. S., additional, Tonini, C., additional, and Zafar, T., additional

Published
2017
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44. The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

Author

Bloom, J. V., primary, Croom, S. M., additional, Bryant, J. J., additional, Callingham, J. R., additional, Schaefer, A. L., additional, Cortese, L., additional, Hopkins, A. M., additional, D'Eugenio, F., additional, Scott, N., additional, Glazebrook, K., additional, Tonini, C., additional, McElroy, R. E., additional, Clark, H. A., additional, Catinella, B., additional, Allen, J. T., additional, Bland-Hawthorn, J., additional, Goodwin, M., additional, Green, A. W., additional, Konstantopoulos, I. S., additional, Lawrence, J., additional, Lorente, N., additional, Medling, A. M., additional, Owers, M. S., additional, Richards, S. N., additional, and Sharp, R., additional

Published
2017
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45. Deriving a multivariate αCO conversion function using the [CII]/CO(1-0) ratio and its application to molecular gas scaling relations

Author

Accurso, G., primary, Saintonge, A., additional, Catinella, B., additional, Cortese, L., additional, Davé, R., additional, Dunsheath, S. H., additional, Genzel, R., additional, Gracia-Carpio, J., additional, Heckman, T. M., additional, Jimmy, Jimmy, additional, Kramer, C., additional, Li, Cheng, additional, Lutz, K., additional, Schiminovich, D., additional, Schuster, K., additional, Sternberg, A., additional, Sturm, E., additional, Tacconi, L. J., additional, Tran, K. V., additional, and Wang, J., additional

Published
2017
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46. The SAMI Galaxy Survey: kinematics of dusty early-type galaxies

Author

Bassett, R., primary, Bekki, K., additional, Cortese, L., additional, Couch, W. J., additional, Sansom, A. E., additional, van de Sande, J., additional, Bryant, J. J., additional, Foster, C., additional, Croom, S. M., additional, Brough, S., additional, Sweet, S. M., additional, Medling, A. M., additional, Owers, M. S., additional, Driver, S. P., additional, Davies, L. J. M., additional, Wong, O. I., additional, Groves, B. A., additional, Bland-Hawthorn, J., additional, Richards, S. N., additional, Goodwin, M., additional, Konstantopoulos, I. S., additional, and Lawrence, J. S., additional

Published
2017
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47. The SAMI Galaxy Survey: the cluster redshift survey, target selection and cluster properties

Author

Owers, M. S., primary, Allen, J. T., additional, Baldry, I., additional, Bryant, J. J., additional, Cecil, G. N., additional, Cortese, L., additional, Croom, S. M., additional, Driver, S. P., additional, Fogarty, L. M. R., additional, Green, A. W., additional, Helmich, E., additional, de Jong, J. T. A., additional, Kuijken, K., additional, Mahajan, S., additional, McFarland, J., additional, Pracy, M. B., additional, Robotham, A. G. S., additional, Sikkema, G., additional, Sweet, S., additional, Taylor, E. N., additional, Verdoes Kleijn, G., additional, Bauer, A. E., additional, Bland-Hawthorn, J., additional, Brough, S., additional, Colless, M., additional, Couch, W. J., additional, Davies, R. L, additional, Drinkwater, M. J., additional, Goodwin, M., additional, Hopkins, A. M., additional, Konstantopoulos, I. S., additional, Foster, C., additional, Lawrence, J. S., additional, Lorente, N. P. F, additional, Medling, A. M., additional, Metcalfe, N., additional, Richards, S. N., additional, van de Sande, J., additional, Scott, N., additional, Shanks, T., additional, Sharp, R., additional, Thomas, A. D., additional, and Tonini, C., additional

Published
2017
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49. The SAMI galaxy survey: exploring the gas-phase mass–metallicity relation.

Author

Sánchez, S F, Barrera-Ballesteros, J K, López-Cobá, C, Brough, S, Bryant, J J, Bland-Hawthorn, J, Croom, S M, van de Sande, J, Cortese, L, Goodwin, M, Lawrence, J S, López-Sánchez, A R, Sweet, S M, Owers, M S, Richards, S N, Walcher, C J, and Team, SAMI

Subjects
INTEGRAL field spectroscopy
Abstract

We present a detailed exploration of the stellar mass versus gas-phase metallicity relation (MZR) using integral field spectroscopy data obtained from ∼1000 galaxies observed by the SAMI galaxy survey. These spatially resolved spectroscopic data allow us to determine the metallicity within the same physical scale (R eff) for different calibrators. The shape of the MZ relations is very similar between the different calibrators, while there are large offsets in the absolute values of the abundances. We confirm our previous results derived using the spatially resolved data provided by the CALIFA and MaNGA surveys: (1) we do not find any significant secondary relation of the MZR with either the star formation rate (SFR) or the specific SFR (SFR/ M *) for any of the calibrators used in this study, based on the analysis of the individual residuals; (2) if there is a dependence with the SFR, it is weaker than the reported one (rc ∼ −0.3), it is confined to the low-mass regime (M * < 109 M⊙) or high-SFR regimes, and it does not produce any significant improvement in the description of the average population of galaxies. The aparent disagreement with published results based on single-fibre spectroscopic data could be due to (i) the interpretation of the secondary relation itself; (ii) the lower number of objects sampled at the low-mass regime by the current study; or (iii) the presence of extreme star-forming galaxies that drive the secondary relation in previous results. [ABSTRACT FROM AUTHOR]

Published
2019
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50. SAMI Galaxy Survey: observing the environmental quenching of star formation in GAMA groups.

Author

Schaefer, A L, Croom, S M, Scott, N, Brough, S, Allen, J T, Bekki, K, Bland-Hawthorn, J, Bloom, J V, Bryant, J J, Cortese, L, Davies, L J M, Federrath, C, Fogarty, L M R, Green, A W, Groves, B, Hopkins, A M, Konstantopoulos, I S, López-Sánchez, A R, Lawrence, J S, and McElroy, R E

Subjects
STAR formation, GALACTIC evolution, STELLAR mass, RADIAL distribution function, DENSITY of stars
Abstract

We explore the radial distribution of star formation in galaxies in the SAMI Galaxy Survey as a function of their Local Group environment. Using a sample of galaxies in groups (with halo masses less than |$\simeq 10^{14} \, \mathrm{M_{\odot }}$|⁠) from the Galaxy And Mass Assembly Survey, we find signatures of environmental quenching in high-mass groups (⁠|$M_{\mathrm{ G}}\, \gt\, 10^{12.5} \, \mathrm{M_{\odot }}$|⁠). The mean integrated specific star formation rate (sSFR) of star-forming galaxies in high-mass groups is lower than for galaxies in low-mass groups or those that are ungrouped, with |$\Delta \log (\mathrm{ sSFR}/\mathrm{yr^{-1}}) \,=\, 0.45 \pm 0.07$|⁠. This difference is seen at all galaxy stellar masses. In high-mass groups, star-forming galaxies more massive than |$M_{*} \sim 10^{10} \, \mathrm{M_{\odot }}$| have centrally concentrated star formation. These galaxies also lie below the star formation main sequence, which suggests they may be undergoing outside-in quenching. Lower mass galaxies in high-mass groups do not show evidence of concentrated star formation. In groups less massive than |$M_{\mathrm{ G}} = 10^{12.5} \, \mathrm{M_{\odot }}$|⁠, we do not observe these trends. In this regime, we find a modest correlation between centrally concentrated star formation and an enhancement in the total star formation rate, consistent with triggered star formation in these galaxies. [ABSTRACT FROM AUTHOR]

Published
2019
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